Astronomy and Astrophysics, volume 400, 223-239 (2003/3-2)
Infrared observations of NGC3603. II. A 11.9µm and 18µm survey.
NUERNBERGER D.E.A. and STANKE T.
Abstract (from CDS):
We present results of the first sub-arcsec resolution mid infrared survey of the southern hemisphere giant HII region NGC 3603. We have observed selected fields in the vicinity of the OB cluster at wavelengths of 11.9µm and 18µm using TIMMI2 mounted on the ESO 3.6m telescope. These fields comprise areas with dense molecular cores, embedded near infrared sources as well as several OH, H2O and CH3OH maser sources, which give indications of ongoing star formation processes. We report the detection of 36 mid infrared point sources and additionally provide flux measurements for 42 knots of diffuse emission. In the area surveyed the protostar IRS 9A is found to be the most luminous source at both 11.9µm and 18µm. Located in its immediate vicinity two more sources (IRS 9B and IRS 9C) also exhibit significant 11.9µm and 18µm emission, thus providing further indications for IRS 9 being an association of protostars in its own right. Several other 11.9µm point sources are related to near infrared sources with strong K-band excess emission and/or to maser sources, which classifies them as young sources, too. In contrast, the second strongest 11.9µm source, IRS 4, appears to be in a more evolved stage. Towards the center of the OB cluster we observe mid infrared emission arising from the three Wolf-Rayet stars WR 43abc, providing evidence for dust production and/or the presence of plasma in their circumstellar envelopes. Spread all over the cluster, we detect a number of sources with mid infrared fluxes close to the sensitivity limit (∼0.01Jy) of our 11.9µm data, which apparently have very red K-N colours. We suggest that these sources are circumstellar disks which are externally heated by the nearby massive stars. Towards the south and west of the OB cluster, large amounts of diffuse emission are found closely correlated with ionized material. We identify at least 7 shocks and ionization fronts, reflecting the enormous impact of the fast stellar winds and ionizing photons, originating from the massive cluster stars, on the adjacent gas and dust. This is impressively emphasized by the shocked and ionized material associated with the heads of the two prominent pillars. Both pillars are easily seen in our 11.9µm and 18µm data: the western one rather prominent in emission, the eastern one more pronounced in absorption against a strong diffuse mid infrared background. Among those sources, for which our data do not reveal any point-like mid infrared counterpart, are IRS1 as well as the three ``proplyds''. However, at least for ``proplyd'' 3 we detect extended, rim-like 11.9µm emission. Therefore, we consider it likely that NGC 3603's ``proplyds'' simply represent scaled-down versions of the neighbouring pillars, i.e. remnant density enhancements of the pristine molecular cloud which to date were able to resist the ionizing and photoevaporating radiation from the nearby OB stars.
surveys - stars: early-type - stars: formation - stars: pre-main sequence - ISM: HII regions - ISM: individual objects: NGC 3603
Table 2: [NS2003] NNA N=77, (Nos 1-48). Table 2: [FPA77] NGC 3603 IRS NNA (Nos 9A-9C) added.
Fig.2: Shock Front SF 1 to SF 7 not in SIMBAD. Table 2: Sher 25 = NGC 3603 25, Stars MTT AN are CL* NGC 3603 BLW AN in SIMBAD.
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